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Paper   IPM / P / 6792
School of Physics
  Title:   Hot Neutron Star Matter Equation of State
1.  N. Riazi
2.  G.H. Bordbar
  Status:   Published
  Journal: Int. J. Theor. Phys., Group Theory and Nonlinear Optics
  No.:  107
  Vol.:  7
  Year:  2001
  Pages:   73-86
  Supported by:  IPM
Free energy per nucleon, nucleonic effective masses, proton fraction, and the equation of state are calculated for hot neutron star matter. Modern AV18 potential is employed in our calculations, together with the older AV14 potential for the sake of comparison. It is shown that the proton fraction decreases as the neutron star matter cools down. It turns out that the AV18 equation of state is considerably stiffer than that of the AV14 potential. The polytropic behavior of the P(ρ) relation and the non-existence of phase transition are also pointed out.

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